Modelling the TSZ power spectrum
The structure formation in university is a hierarchical process. As universe evolves, tiny density fluctuations that existed in the early universe grows under gravitational instability to form massive large scale structures. The galaxy clusters are the massive viralized objects that forms by accreti...
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ftosti:oai:osti.gov:1016115 2023-07-30T04:06:56+02:00 Modelling the TSZ power spectrum Bhattacharya, Suman Shaw, Laurie D Nagai, Daisuke 2021-02-12 application/pdf http://www.osti.gov/servlets/purl/1016115 https://www.osti.gov/biblio/1016115 unknown http://www.osti.gov/servlets/purl/1016115 https://www.osti.gov/biblio/1016115 71 ABUNDANCE COSMOLOGY FLUCTUATIONS GALAXY CLUSTERS GRAVITATIONAL INSTABILITY PHYSICS SIMULATION SKY TELESCOPES UNIVERSE 2021 ftosti 2023-07-11T08:50:06Z The structure formation in university is a hierarchical process. As universe evolves, tiny density fluctuations that existed in the early universe grows under gravitational instability to form massive large scale structures. The galaxy clusters are the massive viralized objects that forms by accreting smaller clumps of mass until they collapse under their self-gravity. As such galaxy clusters are the youngest objects in the universe which makes their abundance as a function of mass and redshift, very sensitive to dark energy. Galaxy clusters can be detected by measuring the richness in optical waveband, by measuring the X-ray flux, and in the microwave sky using Sunyaev-Zel'dovich (SZ) effect. The Sunyaev-Zel'dovich (SZ) effect has long been recognized as a powerful tool for detecting clusters and probing the physics of the intra-cluster medium. Ongoing and future experiments like Atacama Cosmology Telescope, the South Pole Telescope and Planck survey are currently surveying the microwave sky to develop large catalogs of galaxy clusters that are uniformly selected by the SZ flux. However one major systematic uncertainties that cluster abundance is prone to is the connection between the cluster mass and the SZ flux. As shown by several simulation studies, the scatter and bias in the SZ flux-mass relation can be a potential source of systematic error to using clusters as a cosmology probe. In this study they take a semi-analytic approach for modeling the intra-cluster medium in order to predict the tSZ power spectrum. The advantage of this approach is, being analytic, one can vary the parameters describing gas physics and cosmology simultaneously. The model can be calibrated against X-ray observations of massive, low-z clusters, and using the SZ power spectrum which is sourced by high-z lower mass galaxy groups. This approach allows us to include the uncertainty in gas physics, as dictated by the current observational uncertainties, while measuring the cosmological parameters using the SZ power spectrum data. The ... Other/Unknown Material South pole SciTec Connect (Office of Scientific and Technical Information - OSTI, U.S. Department of Energy) South Pole |
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71 ABUNDANCE COSMOLOGY FLUCTUATIONS GALAXY CLUSTERS GRAVITATIONAL INSTABILITY PHYSICS SIMULATION SKY TELESCOPES UNIVERSE |
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71 ABUNDANCE COSMOLOGY FLUCTUATIONS GALAXY CLUSTERS GRAVITATIONAL INSTABILITY PHYSICS SIMULATION SKY TELESCOPES UNIVERSE Bhattacharya, Suman Shaw, Laurie D Nagai, Daisuke Modelling the TSZ power spectrum |
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71 ABUNDANCE COSMOLOGY FLUCTUATIONS GALAXY CLUSTERS GRAVITATIONAL INSTABILITY PHYSICS SIMULATION SKY TELESCOPES UNIVERSE |
description |
The structure formation in university is a hierarchical process. As universe evolves, tiny density fluctuations that existed in the early universe grows under gravitational instability to form massive large scale structures. The galaxy clusters are the massive viralized objects that forms by accreting smaller clumps of mass until they collapse under their self-gravity. As such galaxy clusters are the youngest objects in the universe which makes their abundance as a function of mass and redshift, very sensitive to dark energy. Galaxy clusters can be detected by measuring the richness in optical waveband, by measuring the X-ray flux, and in the microwave sky using Sunyaev-Zel'dovich (SZ) effect. The Sunyaev-Zel'dovich (SZ) effect has long been recognized as a powerful tool for detecting clusters and probing the physics of the intra-cluster medium. Ongoing and future experiments like Atacama Cosmology Telescope, the South Pole Telescope and Planck survey are currently surveying the microwave sky to develop large catalogs of galaxy clusters that are uniformly selected by the SZ flux. However one major systematic uncertainties that cluster abundance is prone to is the connection between the cluster mass and the SZ flux. As shown by several simulation studies, the scatter and bias in the SZ flux-mass relation can be a potential source of systematic error to using clusters as a cosmology probe. In this study they take a semi-analytic approach for modeling the intra-cluster medium in order to predict the tSZ power spectrum. The advantage of this approach is, being analytic, one can vary the parameters describing gas physics and cosmology simultaneously. The model can be calibrated against X-ray observations of massive, low-z clusters, and using the SZ power spectrum which is sourced by high-z lower mass galaxy groups. This approach allows us to include the uncertainty in gas physics, as dictated by the current observational uncertainties, while measuring the cosmological parameters using the SZ power spectrum data. The ... |
author |
Bhattacharya, Suman Shaw, Laurie D Nagai, Daisuke |
author_facet |
Bhattacharya, Suman Shaw, Laurie D Nagai, Daisuke |
author_sort |
Bhattacharya, Suman |
title |
Modelling the TSZ power spectrum |
title_short |
Modelling the TSZ power spectrum |
title_full |
Modelling the TSZ power spectrum |
title_fullStr |
Modelling the TSZ power spectrum |
title_full_unstemmed |
Modelling the TSZ power spectrum |
title_sort |
modelling the tsz power spectrum |
publishDate |
2021 |
url |
http://www.osti.gov/servlets/purl/1016115 https://www.osti.gov/biblio/1016115 |
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South Pole |
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South pole |
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South pole |
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http://www.osti.gov/servlets/purl/1016115 https://www.osti.gov/biblio/1016115 |
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1772819905041661952 |